coverpage: title_1: THE STELLAR CONTENT OF WOLF-RAYET GALAXIES(FOS SPECTRA) sci_cat: STELLAR POPULATIONS sci_subcat: YOUNG FIELD STARS proposal_for: GO/CAR cont_id: 4122 pi_title: DR. pi_fname: PETER pi_mi: S. pi_lname: CONTI pi_inst: JILA pi_country: USA pi_phone: (303) 492-8497 keywords_1: LBV'S, WOLF-RAYET STARS, STARBURSTS hours_pri: 12.4 num_pri: 18 fos: Y pi_position: ASTRONOMER off_fname: LAURENCE off_mi: D. off_lname: NELSON off_title: DIR/OCG off_inst: THE REGENTS OF THE UNIVERSITY OF COLORADO off_addr_1: BOX 19 off_addr_2: UNIVERSITY OF COLORADO off_city: BOULDER off_state: CO off_zip: 803090019 off_country: USA off_phone: (303) 492-6221 ! end of coverpage abstract: line_1: We propose to observe a comprehensive sample of Wolf-Rayet (W-R) galaxies line_2: --- starburst galaxies in which broad 4686 He II emission of stellar line_3: origin has been detected. These galaxies generally contain far more W-R line_4: stars than the Milky Way, M31, and other normal galaxies. The ultraviolet line_5: FOC images and FOS spectra will be combined with optical and infrared line_6: data as part of a large effort to perform a broad, systematic analysis line_7: of the properties of W-R galaxies. The UV data obtained with HST will line_8: provide crucial constraints on the hot star (O and W-R) populations, and line_9: will lead to a better understanding of the physical conditions, initial line_10: mass functions, and starburst parameters of these galaxies. The overall line_11: continuum will be analyzed within the framework of evolutionary and line_12: spectral synthesis models that we are developing. Quantitative line_13: spectroscopy of UV resonance lines will allow us to study the hot star line_14: populations in detail, and to directly measure the number of OB stars line_15: within these galaxies. Our main goal is to determine which physical line_16: properties of W-R galaxies (e.g., IMF slope, chemical composition, age, line_17: strength and duration of the starburst) have led to the production of line_18: large numbers of W-R stars. The results of this study will have line_19: important implications for our understanding of W-R galaxies,and also line_20: of starburst and emission-line galaxies in general. ! ! end of abstract general_form_proposers: lname: CONTI fname: PETER title: PI mi: S. inst: UNIVERSITY OF COLORADO country: USA ! lname: FILIPPENKO fname: ALEXEI mi: V. inst: UNIVERSITY OF CALIFORNIA, BERKELEY country: USA ! lname: LEITHERER fname: CLAUS inst: SPACE TELESCOPE SCIENCE INSTITUTE country: USA esa: Y ! lname: ROBERT fname: CARMELLE inst: SPACE TELESCOPE SCIENCE INSTITUTE country: USA ! lname: SARGENT fname: WALLACE mi: L. inst: CALIFORNIA INSTITUTE OF TECHNOLOGY country: USA ! lname: VACCA fname: WILLIAM mi: D. inst: UNIVERSITY OF CALIFORNIA, BERKELEY country: USA ! ! end of general_form_proposers block general_form_text: question: 3 section: 1 line_1: We would like to obtain FOS spectra of the brightest knots of line_2: some W-R galaxies. The objects were selected on the basis of the FOC line_3: data from another proposal; There may be more than one knot per galaxy. line_4: The scientific goal can be best achieved with the FOS and gratings line_5: G130H and G190H. We intend to use the blue-side detector for both line_6: gratings. A peak-up technique is used for the TA. ! question: 4 section: 1 line_1: It is the combination of the superior resolution (IUE: 6A; FOS: 3A for line_2: a knot of 2-3") and vastly better S/N (IUE: typically 10; FOS: 35 for line_3: our proposed observations) of HST data which provide a dramatic line_4: improvement. STRONG lines (like C IV) can be modeled quantitatively line_5: with HST, and WEAKER lines (like N IV 1718, which is an important line_6: signature of hot EVOLVED stars) can only be detected with HST, in line_7: contrast to IUE. ! question: 6 section: 1 line_1: No special calibrations are requested. According to the FOC instrument line_2: scientist, PSF's will be provided by STScI. ! question: 7 section: 1 line_1: The general management of the observations (including the ground line_2: observations) and the data reduction and interpretation will be line_3: coordinated by Peter Conti. line_4: FOS deconvolution will be carried out by Claus Leitherer. P. Conti is line_5: also in charge of the pre-analysis of the HST observations (line line_6: identification, interstellar extinction...). Other observations from line_7: the ground are to be acquired, reduced and analysed by Alex Filippenko, line_8: Wal Sargent and Bill Vacca. line_9: The population synthesis models will be done at STScI by Carmelle line_10: Robert and Claus Leitherer. All co-Is will be intimately involved with line_11: data analysis and interpretation. ! question: 8 section: 1 line_1: The HST observations are supported by ground-based observations. There line_2: is no need for simultaneous observations. ! !end of general form text general_form_address: lname: CONTI fname: PETER mi: S title: DR. category: PI inst: JILA/UNIV. OF COLORADO addr_1: CAMPUS BOX 440 city: BOULDER state: CO zip: 80309 country: USA phone: (303) 492-8497 telex: 755842 JILA ! ! end of general_form_address records fixed_targets: targnum: 10 name_1: NGC1741-OFFSET descr_1: E,318,928 pos_1: RA=5H 01M 37.73S +/- 0.05S, pos_2: DEC=-4D 15' 28.73" +/-0.5" equinox: 2000 pos_epoch_bj: J pos_epoch_yr: 1990.00 acqpr_1: EXT fluxval_1: F(2200)=2.4 E-15 targnum: 20 name_1: NGC1741B descr_1: E,318,928 pos_1: RA=5H 01M 37.70S +/- 0.05S, pos_2: DEC=-4D 15' 32.55" +/-0.5" equinox: 2000 pos_epoch_bj: J pos_epoch_yr: 1990.00 acqpr_1: EXT fluxval_1: F(2200)=2.0 E-15 ! ! end of fixed targets ! No solar system records found ! No generic target records found exposure_logsheet: linenum: 100.000 targname: NGC1741-OFFSET config: HRS opmode: ACQ aperture: 2.0 sp_element: MIRROR-N2 num_exp: 1 time_per_exp: 250S priority: 1 param_1: SEARCH-SIZE=5 param_2: BRIGHT=RETURN req_1: CYCLE 4; req_2: ONBOARD ACQ FOR 101; req_3: SEQ 100-204 NO GAP comment_1: STEP-TIME=10S ! linenum: 101.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G140L wavelength: 1320 num_exp: 1 time_per_exp: 60S priority: 1 req_1: CYCLE 4; req_2: CALIB FOR 102; ! linenum: 102.000 targname: NGC1741-OFFSET config: HRS opmode: ACCUM aperture: 2.0 sp_element: G140L wavelength: 1320 num_exp: 1 time_per_exp: 6100S priority: 1 req_1: CYCLE 4; ! linenum: 103.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G140L wavelength: 1600 num_exp: 1 time_per_exp: 60S priority: 1 req_1: CYCLE 4; req_2: CALIB FOR 104; linenum: 104.000 targname: NGC1741-OFFSET config: HRS opmode: ACCUM aperture: 2.0 sp_element: G140L wavelength: 1600 num_exp: 1 time_per_exp: 12200S priority: 1 req_1: CYCLE 4; ! linenum: 201.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G140L wavelength: 1320 num_exp: 1 time_per_exp: 60S priority: 1 req_1: CYCLE 4; req_2: CALIB FOR 202; comment_1: BLIND OFFSET FROM NGC1741-OFFSET; ! linenum: 202.000 targname: NGC1741B config: HRS opmode: ACCUM aperture: 2.0 sp_element: G140L wavelength: 1320 num_exp: 1 time_per_exp: 6100S priority: 1 req_1: CYCLE 4; comment_1: BLIND OFFSET FROM NGC1741-OFFSET; ! linenum: 203.000 targname: WAVE config: HRS opmode: ACCUM aperture: SC2 sp_element: G140L wavelength: 1600 num_exp: 1 time_per_exp: 60S priority: 1 req_1: CYCLE 4; req_2: CALIB FOR 204; comment_1: BLIND OFFSET FROM NGC1741-OFFSET; linenum: 204.000 targname: NGC1741B config: HRS opmode: ACCUM aperture: 2.0 sp_element: G140L wavelength: 1600 num_exp: 1 time_per_exp: 12200S priority: 1 req_1: CYCLE 4; comment_1: BLIND OFFSET FROM NGC1741-OFFSET; !! end of exposure logsheet ! No scan data records found